Table 3: Microturbulence determinations from Fe I and Fe II lines.
    Number $\xi_{1}$   $\xi_{2}$    
Star Species of Lines (km s-1) $\log N/N_{\rm T}$ (km s-1) $\log N/N_{\rm T}$ gf values
$\theta$ And Fe I 34 3.9 $-4.27\pm0.28$ 3.9 $-4.27\pm0.28$ MF + KX
  Fe II 23 3.2 $-4.22\pm0.24$ 3.2 $-4.22\pm0.24$ MF + KX
    adopted 3.6        
$\epsilon$ Del Fe II 32 0.0 $-4.56\pm0.21$ 0.0 $-4.56\pm0.21$ MF + KX
    adopted 0.0        
$\epsilon$ Aqr Fe I 33 3.1 $-4.66\pm0.25$ 3.1 $-4.66\pm0.25$ MF + KX
  Fe II 24 2.4 $-4.60\pm0.26$ 2.5 $-4.62\pm0.24$ MF+KX
    adopted 2.8        
$\iota$ And Fe II 44 1.3 $-4.71\pm0.19$ 1.2 $-4.69\pm0.19$ MF + KX
  Fe II 34 1.4 $-4.75\pm0.20$ 1.4 $-4.75\pm0.20$ MF
    adopted 1.3        

gf value references: MF = Fuhr et al. (1988), KX = Kurucz & Bell (1995).
Note: For $\xi_{1}$ and $\xi_{2}$ the abundances are found so that there is no trend of values for lines of different equivalent widths and have minimum scatter about the mean, respectively.

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